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Radioisotopic ages for meteorites and their components provide constraints onthe evolution of small bodies: timescales of accretion, thermal and aqueousmetamorphism, differentiation, cooling and impact metamorphism. Realising thatthe decay heat of short-lived nuclides (e.g. 26Al, 60Fe), was the main heatsource driving differentiation and metamorphism, thermal modeling of smallbodies is of utmost importance to set individual meteorite age data into thegeneral context of the thermal evolution of their parent bodies, and to derivegeneral conclusions about the nature of planetary building blocks in the earlysolar system. As a general result, modelling easily explains that ironmeteorites are older than chondrites, as early formed planetesimals experienceda higher concentration of short-lived nuclides and more severe heating.However, core formation processes may also extend to 10 Ma after formation ofCalcium-Aluminum-rich inclusions (CAIs). A general effect of the porous natureof the starting material is that relatively small bodies (< few km) will alsodifferentiate if they form within 2 Ma after CAIs. A particular interestingfeature to be explored is the possibility that some chondrites may derive fromthe outer undifferentiated layers of asteroids that are differentiated in theirinteriors. This could explain the presence of remnant magnetization in somechondrites due to a planetary magnetic field.

Early Thermal Evolution of Planetesimals and its Impact on Processing and Dating of Meteoritic Material